To summarize, the orbital motion scenario fails to account for the properties of the
knot spatial distribution in the Cep E protostellar jet. Our analysis favors a jet precession scenario as origin of the outflow wiggles. As mentioned above in this Section, [1]} proposed that jet precession originates in the tidal interaction between the protostellar disk driving the jet and a non-coplanar binary companion. The authors applied their analytic model to the case of Cep E based on the parameters estimated by [2]}. They concluded that the system is a very close binary with a distance in the range 4 – 20 au and a small disk radius R= 1 – 10 au. Taking into account the much longer precession timescale implied by our new model, \(2000\hbox{\hspace{1.99997pt}yr}\)  instead of \(400\hbox{\hspace{1.99997pt}yr}\) , the separation of the binary increases by a factor \(\sim 2\)  up to 8 – 40 au (001 – 005) but unfortunately the linear scales involved remain out of reach to the NOEMA interferometer.
We note that also in the scenario proposed by [1]}, protostar B cannot be responsible for the precession observed in the jet from protostar A.
